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Solar System
Suryadi Siregar
Prodi AstronomiITB
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Approximate Typical
Conditions in Galaxy
Region of Interstellar Space
Within our Galaxy
Number Density,
Atoms / cm3
Temperature,*
Kelvins
Inside our Heliosphere,
in the Vicinity of Earth5 10,000
Local Cloud Surrounding
our Heliosphere0.3 7,000
Nearby Void (Local Bubble) < 0.001 1,000,000Typical Star-Forming Cloud >1,000 100
Best Laboratory Vacuum 1000
Classroom Atmosphere 2.7 X 1019 288
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Evolution of Solar SystemTheory of Nebular Contraction
Pioneers: Rene de Cartes(1644),
Pierre Simon de Laplace(1796),
Immanuel Kant..
Start with a sphere of gas that is
rotating and contracting, that hasradius of 104Ro, a mean density of
10-12o
contract and rotate until it collapse
into a disk. Central part became the
Sun. Others to be planets Early stages (above). Late stages
(below)
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eory o ose ncoun ers etidal Theories)
Pioneers: Georges Louis
de Buffon, Chamberlain
.
Summary: Closestencounter of the stars
attracts the matter of each
stars. Formation of the
planets by thecondensation of material
lost from each star. The
planet revolve the stars
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Theory of Nebular Cluster
The nebula contracts under the
influence of gravitation,
rotational velocity increases
until it collapse into a disk Most massive nebula
concentrate in the center. Mass
density increase, temperature
augmented Sun was born ! Less massive matter ejected to
edge. Forming the planets and
small bodies in solar system
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The Solar System Disc Clearance
After the formation of theSun. The residue of matter
continue to rotate, contract
and revolve around the Sun
In early stage thedistribution of matter in the
solar system relatively
homogeny
Step by step theinterplanetary-matter
agglomerates to form the
planets/ protoplanets
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Mass Distribution Within the
Solar System
99.85% Sun
0.135% Planets
0.015% Comets
Kuiper belt objects
Satellites of the planets
Minor Planets (Asteroids)
MeteoroidsInterplanetary Medium
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Residual of primitive cloud
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Jupiter Saturn
Uranus
Neptune
Pluto
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Inferior Planets (r1
AU): high eccentricity,
low density
(Mars, Jupiter, Saturn,
Uranus and Neptune)
Criteria:
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The small and rocky planet Mercury is the closest planet to the Sun; it speeds
around the Sun in a wildly elliptical (non-circular) orbit that takes it as close as 47
million km and as far as 70 million km from the Sun. Mercury completes a trip
around the Sun every 88 days, speeding through space at nearly 50 km per
second, faster than any other planet. Because it is so close to the Sun,temperatures on its surface can reach 467 degrees Celsius. But because the
planet has hardly any atmosphere to keep it warm, nighttime temperatures can
drop to -183 degrees Celsius.
Because Mercury is so close to the Sun, it is hard to see from Earth except during
twilight. Until 1965, scientists thought that the same side of Mercury always facedthe Sun. Then, astronomers discovered that Mercury completes three rotations for
every two orbits around the Sun. The length of one Mercury day (sidereal rotation)
is equal to 58.646 Earth days
Mercury
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Venus
At first glance, if Earth had a twin, it would be Venus. The two planets are similar
in size, mass, composition, and distance from the Sun. But there the similarities
end. Venus has no ocean. Venus is covered by thick, rapidly spinning clouds that
trap surface heat, creating a scorched greenhouse-like world with temperatures
hot enough to melt lead and pressure so intense that standing on Venus would
feel like the pressure felt 900 meters deep in Earth's oceans. These clouds
reflect sunlight in addition to trapping heat. Because Venus reflects so much
sunlight, it is usually the brightest planet in the sky.
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Earth:
Some facts are well known. For instance, Earth is the third planet from the Sun and the
fifth largest in the solar system. Earth's diameter is just a few hundred kilometers larger
than that ofVenus. The four seasons are a result of Earth's axis of rotation being tilted
more than 23 degrees.
The regular daily and monthly rhythms ofEarth's only natural satellite, the Moon, haveguided timekeepers for thousands of years. Its influence on Earth's cycles, notably tides,
has also been charted by many cultures in many ages. More than 70 spacecraft have
been sent to the Moon; 12 astronauts have walked upon its surface and brought back
382 kg (842 pounds) of lunar rock and soil to Earth.
How did the Moon come to be? The leading theory is that a Mars-sized body once hitEarth and the resulting debris (from both Earth and the impacting body) accumulated to
form the Moon. Scientists believe that the Moon was formed approximately 4.5 billion
years ago (the age of the oldest collected lunar rocks). When the Moon formed, its outer
layers melted under very high temperatures, forming the lunar crust, probably from a
global "magma ocean."
http://solarsystem.nasa.gov/planets/profile.cfm?Object=Venushttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Earthhttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Marshttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Marshttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Marshttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Marshttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Earthhttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Venus -
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Earths Atmosphere
Consists of 5 layers( function oftemperature gradient)
Troposphere
Stratosphere
Mesosphere
ThermosphereExosphere
Composition
-N2 78.084 %
-O2
20.946 %
-A 0.934 %
-CO2 0.035 %
ux1.e
iu.edu
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Mars
Mars is a small rocky body once thought to be very Earth-like. Like the
other "terrestrial" planets - Mercury, Venus, and Earth - its surface has
been changed by volcanism, impacts from other bodies, movements of its
crust, and atmospheric effects such as dust storms. It has polar ice caps
that grow and recede with the change of seasons; areas of layered soils
near the Martian poles suggest that the planet's climate has changed
more than once, perhaps caused by a regular change in the planet's orbit.
Martian tectonics - the formation and change of a planet's crust - differs
from Earth's. Where Earth tectonics involve sliding plates that grind
against each other or spread apart in the seafloors, Martian tectonicsseem to be vertical, with hot lava pushing upwards through the crust to the
surface. Periodically, great dust storms engulf the entire planet. The
effects of these storms are dramatic, including giant dunes, wind streaks,
and wind-carved features
http://solarsystem.nasa.gov/planets/profile.cfm?Object=Mercuryhttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Venushttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Earthhttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Earthhttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Venushttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Mercury -
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Mars Atmosphere
Very massive approximately
100x Earths atmosphere
Composition:
-CO2 = 96.5%
-N2 = 3.5%
-SO2 =0.02%
-A = 0.007%
-Ne = 0.001%
Sulfuric acid of cloud and haze
at 30 up to 80 km
physics.uoregon.edu
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Martian soils insitu exploration
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Phobos and Deimos
Asaph Hall,1877
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Main-Belt Asteroids
Sphere of gravitation influence
Scenario the formation of
Phobos and Deimos
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Sphere of gravitation influence
25m
R r
M
R=radius of sphere of influence by a planet
r=heliocentric distance
M=mass of the Sun, m=mass of the planet,
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No Parameter Phobos Deimos
1 r[km] 9377 23436
2 P[day] 0.31891 1.262443 a[km] 26 12
4 b[km] 18 10
5 M[1015kg] 10.8 1.8
6 [kg/m3] 1900 1750
Table . Physical and orbital data of Phobos and Demos
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JupiterThe most massive planet in our solar system, with four planet-sized moons and many
smaller moons, Jupiter forms a kind of miniature solar system. Jupiter resembles astar in composition. In fact, if it had been about eighty times more massive, it would
have become a star rather than a planet.
On January 7, 1610, using his primitive telescope, astronomer Galileo Galilee saw
four small 'stars' near Jupiter. He had discovered Jupiter's four largest moons, now
called Io, Europa, Ganymede, and Callisto. Collectively, these four moons are knowntoday as the Galilean satellites.
Galileo would be astonished at what we have learned about Jupiter and its moons in
the past 30 years. Io is the most volcanically active body in our solar system.
Ganymede is the largest planetary moon and is the only moon in the solar system
known to have its own magnetic field. A liquid ocean may lie beneath the frozen crustof Europa. Icy oceans may also lie deep beneath the crusts of Callisto and
Ganymede. In 2003 alone, astronomers discovered 23 new moons orbiting the giant
planet, giving Jupiter a total moon count of 63 - the most in the solar system. The
numerous small outer moons may be asteroids captured by the giant planet's gravity
http://solarsystem.nasa.gov/planets/profile.cfm?Object=Jup_Europahttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Jup_Callistohttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Jup_Callistohttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Jup_Europa -
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SaturnSaturn was the most distant of the five planets known to the ancients. In 1610,
Italian astronomer Galileo Galilei was the first to gaze at Saturn through a
telescope. To his surprise, he saw a pair of objects on either side of the planet.
He sketched them as separate spheres and wrote that Saturn appeared to be
triple-bodied. Continuing his observations over the next few years, Galileo drew
the lateral bodies as arms or handles attached to Saturn. In 1659, Dutch
astronomer Christian Huygens, using a more powerful telescope than Galileo's,
proposed that Saturn was surrounded by a thin, flat ring. In 1675, Italian-born
astronomer Jean-Dominique Cassini discovered a 'division' between what are
now called the A and B rings. It is now known that the gravitational influence of
Saturn's moon Mimas is responsible for the Cassini Division, which is 4,800
kilometers (3,000 miles) wide.
Like Jupiter, Saturn is made mostly of hydrogen and helium. Its volume is 755times greater than that of Earth. Winds in the upper atmosphere reach 500
meters (1,600 feet) per second in the equatorial region. (In contrast, the
strongest hurricane-force winds on Earth top out at about 110 meters, or 360
feet, per second.) These super-fast winds, combined with heat rising from within
the planet's interior, cause the yellow and gold bands visible in the atmosphere.
http://solarsystem.nasa.gov/planets/profile.cfm?Object=Jupiterhttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Jupiter -
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How did the ring of the planet
formed? Roches limit (d)
13
1
2
d 2.5 R
R=radius of planet.
1
= density of planet
2 = density of satellite
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1.Consider an orbiting mass of fluid held together
by gravity, here viewed from above the orbitalplane. Far from the Roche limit the mass is
practically spherical.
http://en.wikipedia.org/wiki/File:Roche_limit_(far_away_sphere).PN -
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2. Closer to the Roche limit the
body is deformed by tidal force
http://en.wikipedia.org/wiki/File:Roche_limit_(tidal_sphere).PN -
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3.Within the Roche limit the mass's
own gravity can no longer withstandthe tidal forces, and the body
disintegrates.
http://en.wikipedia.org/wiki/File:Roche_limit_(ripped_sphere).PN -
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4.Particles closer to the primary
move more quickly than particlesfarther away, as represented by the
red arrows.
http://en.wikipedia.org/wiki/File:Roche_limit_(top_view).PN -
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5.The varying orbital speed of thematerial eventually causes it to
form a ring.
http://en.wikipedia.org/wiki/File:Roche_limit_(ring).PN -
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Tidal effects on Io
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Table . Roches Limit for planet-satellite system
No Body Satellite Roche Limit(rigid)
[R]
Roche Limit(fluid)
[R]
1 Earth-Moon 1.49 2.86
2 Earth-Comet 2.80 5.39
3 Sun-Earth 0.80 1.53
4 Sun-Jupiter 1.28 2.46
5 Sun-Moon 0.94 1.81
6 Sun-Comet 1.78 3.42
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Table. Radius of Saturns ring (R=60332 km)
No Name Radius [R] Width
[km]
Thick
[km]
Mass
[kg]
Albedo
1 D 1.235 8500
2 C 1.525 17500 1.1 1021 0.1-0,3
3 B 1.949 25500 0.1-1 2.8 1022 0.4-0,6
4 Cassini
Divission
2.025 4700 5.7 1017 0.2-0,4
5 A 2.267 14600 0.1-1 6.2 1021 0.4-0,6
6 F 2.324 30-500 0.6
7 G 2.748 8000 100-
1000
1 1017
8 E 2.983 300000 1000-
30000
7 108
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Uranus
Once considered one of the blander-looking planets, Uranus has been revealed as a
dynamic world with some of the brightest clouds in the outer solar system and 11
rings. The first planet found with the aid of a telescope, Uranus was discovered in
1781 by astronomer William Herschel. The seventh planet from the Sun is so distant
that it takes 84 years to complete one orbit. Uranus, with no solid surface, is one of
the gas giant planets (the others are Jupiter, Saturn, and Neptune).
The atmosphere of Uranus is composed primarily of hydrogen and helium, with a
small amount of methane and traces of water and ammonia. Uranus gets its blue-
green color from methane gas. Sunlight is reflected from Uranus' cloud tops, which
lie beneath a layer of methane gas. As the reflected sunlight passes back throughthis layer, the methane gas absorbs the red portion of the light, allowing the blue
portion to pass through, resulting in the blue-green color that we see. The planet's
atmospheric details are very difficult to see in visible light. The bulk (80 per-cent or
more) of the mass of Uranus is contained in an extended liquid core consisting
primarily of 'icy' materials (water, methane, and ammonia), with higher-density
material at depth.
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Neptune
The eighth planet from the Sun, Neptune was the first planet located throughmathematical predictions rather than through regular observations of the sky.
(Galileo had recorded it as a fixed star during observations with his small
telescope in 1612 and 1613.) When Uranus didn't travel exactly as astronomers
expected it to, a French mathematician, Urbain Joseph Le Verrier, proposed the
position and mass of another as yet unknown planet that could cause the
observed changes to Uranus' orbit. After being ignored by French astronomers, LeVerrier sent his predictions to Johann Gottfried Galle at the Berlin Observatory,
who found Neptune on his first night of searching in 1846. Seventeen days later,
its largest moon, Triton, was also discovered.
Nearly 4.5 billion kilometers (2.8 billion miles) from the Sun, Neptune orbits the
Sun once every 165 years. It is invisible to the naked eye because of its extremedistance from Earth. Interestingly, due to Pluto's unusual elliptical orbit, Neptune is
actually the farthest planet from the Sun for a 20-year period out of every 248
Earth years
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Comet
Throughout history, people have been both awed and alarmed by comets, starswith "long hair" that appeared in the sky unannounced and unpredictably. We now
know that comets are dirty-ice leftovers from the formation of our solar system
around 4.6 billion years ago. They are among the least-changed objects in our
solar system and, as such, may yield important clues about the formation of our
solar system. We can predict the orbits of many of them, but not all.
Around a dozen "new" comets are discovered each year. Short-period comets are
more predictable because they take less than 200 years to orbit the Sun. Most
come from a region of icy bodies beyond the orbit ofNeptune. These icy bodies are
variously called Kuiper Belt Objects, Edgeworth-Kuiper Belt Objects, or trans-
Neptunian objects. Less predictable are long-period comets, many of which arrive
from a distant region called the Oort cloud about 100,000 astronomical units (thatis, 100,000 times the mean distance between Earth and the Sun) from the Sun.
These comets can take as long as 30 million years to complete one trip around the
Sun. (It takes Earth only 1 year to orbit the Sun.) As many as a trillion comets may
reside in the Oort cloud, orbiting the Sun near the edge of the Sun's gravitational
influence.
http://solarsystem.nasa.gov/planets/profile.cfm?Object=Neptunehttp://solarsystem.nasa.gov/planets/profile.cfm?Object=KBOshttp://solarsystem.nasa.gov/planets/profile.cfm?Object=KBOshttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Neptune -
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Kuiper Belt Object
The Kuiper Belt is often called our Solar System's 'finalfrontier.' This disk-shaped region of icy debris is about 4.5 to
7.5 billion km (2.8 billion to 4.6 billion miles), 30 to 50
Astronomical Units (AU). from our Sun. Its existence
confirmed only a decade ago, the Kuiper Belt and itscollection of icy objects - KBOs - are an emerging area of
research in planetary science.
No spacecraft has ever traveled to the Kuiper Belt, but
NASA's New Horizons mission, planned to arrive at Pluto in
2015, might be able to penetrate farther into the Kuiper Belt
to study one of these mysterious objects.
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Dwarfs Planet
What Defines a Planet?
What constitutes a planet? The International Astronomical Union (IAU) developed somedefinitions in 2001, modified them again in 2003, and as of August 24, 2006, the IAU has
come up with another definition. The IAU said in a statement that the definition for a planet
is now officially known as "a celestial body that (a) is in orbit around the Sun, (b) has
sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a
hydrostatic equilibrium (nearly round) shape and (c) has cleared the neighborhood around
its orbit."
A "dwarf planet" is a celestial body that (a) is in orbit around the Sun, (b) has sufficient mass
for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium
(nearly round) shape, (c) has not cleared the neighborhood around its orbit, and (d) is not a
satellite.
All other objects except satellites orbiting the Sun shall be referred to collectively as "SmallSolar-System Bodies". According to the IAU, more dwarf planets are expected to be
announced in the coming months and years. Currently, a dozen candidate dwarf planets are
listed on IAU's dwarf planet watch list, which keeps changing as new objects are found and
the physics of the existing candidates becomes better-known.
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Oort Cloud
The Oort Cloud is an immense spherical cloud surrounding our Solar System.Extending about 30 trillion kilometers (18 trillion miles) from the Sun, it was first
proposed in 1950 by Dutch astronomer Jan Oort. The vast distance of the Oort
cloud is considered to be the outer edge of the Solar System - where the Sun's
orb of physical and gravitational influence ends.
The Oort Cloud contains billions of icy bodies in solar orbit. Occasionally,
passing stars disturb the orbit of one of these bodies, causing it to comestreaking into the inner solar system as a long-period comet. These comets have
very large orbits and are observed in the inner solar system only once. In
contrast, short-period comets take less than 200 years to orbit the Sun and they
travel along the plane in which most of the planets orbit. They come from a
region beyond Neptune called the Kuiper Belt, named for astronomer Gerard
Kuiper, who proposed its existence in 1951.
In 1991 radio astronomers detected the first extra solar planets orbiting a dying
pulsar star. Although the deadly radiation from the pulsar is not condusive to life,
it was the first example of a star other than our Sun producing planets.
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PlutoStory of Pluto:
On August 24, 2006, the International Astronomical Union (IAU) formally downgraded Plutofrom an official planet to a dwarf planet. According to the new rules a planet meets three
criteria: it must orbit the Sun, it must be big enough for gravity to squash it into a round ball,and it must have cleared other things out of the way in its orbital neighborhood. The lattermeasure knocks out Pluto and 2003UB313 (Eris), which orbit among the icy wrecks of the
Kuiper Belt, and Ceres, which is in the asteroid belt.
(1) A "planet" is a celestial body that (a) is in orbit around the Sun, (b) has sufficient mass for itsself-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly
round) shape, and (c) has cleared the neighborhood around its orbit.
(2) A "dwarf planet" is a celestial body that (a) is in orbit around the Sun, (b) has sufficient massfor its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium(nearly round) shape, (c) has not cleared the neighborhood around its orbit, and (d) is not a
satellite.
(3) All other objects except satellites orbiting the Sun shall be referred to collectively as "SmallSolar-System Bodies".
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Main Belt and Trojan Asteroid
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Formation of Asteroids
1. Forming by the rest of
primordial cloud that
cannot became a
planet. Criteria;
spherical form, low
eccentricity, orbit
relatively stable.
Founded between
Mars and Jupiter
2. Forming by collision
between asteroid inmain belt. Criteria;
irregular form, orbit not
stable, high
eccentricity, crosser
orbit of the planet
Lagrangian Points=Equilibrium position
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Since the invention of the telescope, three more planets have been
discovered in our solar system: Uranus (1781), Neptune (1846), and Pluto(1930). [Now Pluto's status as a "dwarf planet".] In addition, there are
thousands of small bodies such as asteroids and comets. Most of the
asteroids orbit in a region between the orbits ofMars and Jupiter, while the
home of comets lies far beyond the orbit of Pluto, in the Oort Cloud.
The four planets closest to the Sun - Mercury, Venus, Earth, and Mars - arecalled the terrestrial planets because they have solid rocky surfaces. The
four large planets beyond the orbit of Mars - Jupiter, Saturn, Uranus, and
Neptune - are called gas giants. Tiny, distant, Pluto has a solid but icier
surface than the terrestrial planets.
f
http://solarsystem.nasa.gov/planets/profile.cfm?Object=Uranushttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Neptunehttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Plutohttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Asteroidshttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Cometshttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Marshttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Sunhttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Mercuryhttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Venushttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Earthhttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Jupiterhttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Saturnhttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Saturnhttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Jupiterhttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Earthhttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Venushttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Mercuryhttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Sunhttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Marshttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Cometshttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Asteroidshttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Plutohttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Neptunehttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Uranus -
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Revolution and Rotation of
the Earth
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Global Warming
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Milankovitch CycleMilankovitch cycles are the collective effect of changes in the Earth's
movements upon its climate, named after Serbian civil engineer and
mathematician Milutin Milankovi. The eccentricity, axial tilt, and precession of
the Earth's orbit vary in several patterns, resulting in 100,000-year ice age cycles
of the Quaternary glaciation over the last few million years. The Earth's axis
completes one full cycle of precession approximately every 26,000 years. At the
same time, the elliptical orbit rotates, more slowly, leading to a 21,000-year cycle
between the seasons and the orbit. In addition, the angle between Earth'srotational axis and the normal to the plane of its orbit moves from 22.1 degrees
to 24.5 degrees and back again on a 41,000-year cycle. Currently, this angle is
23.44 degrees and is decreasing.
The Milankovitch theory of climate change is not perfectly worked out; in
particular, the largest observed response is at the 100,000-year timescale, but
the forcing is apparently small at this scale, in regard to the ice ages. Variousfeedbacks (from carbon dioxide, or from ice sheet dynamics) are invoked to
explain this discrepancy.
Milankovitch-like theories were advanced by Joseph Adhemar, James Croll and
others, but verification was difficult due to the absence of reliably dated evidence
and doubts as to exactly which periods were important.
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Oort cloud, Kohoutek
orbit ,Gaspra asteroid
and Neat comet
Short-period comets: P< 200
yrs. Elliptical orbit
Long-period comets: P>200
yrs. Orbit: elliptical,parabolic or
hyperbolic
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S d M
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Second Moon
Category Near-Earth asteroid,
Venus-crosser asteroid,
Mars-crosser asteroid
Orbital Epoch May 14, 2008 Aphelion=1.51AU.Perihelion=0.484
AU.Semi-major axis=0.998 AU.Eccentricity=0.515.Orbital
period=363.99 d Average orbital speed=27.73 km/s Meananomaly=134.76. Inclination=19.81.Longitude of
ascending node= 126.28Argument of perihelion= 43.74
Physical Diameter~5 km. Mass=1.31014 kg. Mean density= 2 ?
g/cm. Equatorial surface gravity = 0.0014 m/s . Escapevelocity= 0.0026 km/s. Rotation period= 27.44 h Albedo=
0.15 ?. Temperature~275 K. Spectral type?. Absolute
magnitude (H)=15.1
http://en.wikipedia.org/wiki/File:Orbits_of_Cruithne_and_Earth.gifhttp://en.wikipedia.org/wiki/File:Orbits_of_Cruithne_and_Earth.gifhttp://en.wikipedia.org/wiki/File:Orbits_of_Cruithne_and_Earth.gifhttp://en.wikipedia.org/wiki/File:Orbits_of_Cruithne_and_Earth.gifhttp://en.wikipedia.org/wiki/File:Horseshoe_orbit_of_Cruithne_from_the_perspective_of_Earth.gifhttp://en.wikipedia.org/wiki/File:Orbits_of_Cruithne_and_Earth.gif -
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1898 -> First Amor
1976 -> First Aten
Near Earth Asteroids (NEAs):Amors, Apollos, and Atens
Source: Main belt and Mars-crossers
Near Earth Objects (NEOs)
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Near-Earth Objects (NEOs)
T i l
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1-Opposition
2-Quadrature Western
3-Quadrature Eastern
4-Superior Conjunction
5-Superior Conjunction
6-Maximum Elongation(Western)
7-Maximum Elongation
(Eastern)
8-Inferior ConjunctionEarths Orbit
5
4
3
2
1
Inferior Planet
Superior Planet
Terminology
8Earth
7
6
5
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In the Universe of Kepler & Newton
Planets move on ellipses around Sun
space is flat:
Gravity is interaction between masses
O bit l l E li ti l
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Orbital plane-Ecliptic plane
Ecliptic plane
Orbital plane
North
iPlanet(r,)
Sun
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57
2
2
221
m
Ehe
)(1
)1( 2
eCos
ear
GM
)211(22
arGMV
h = 2 x area/unit time =
Keplers constant
The Orbit-1
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)(1
)1( 2
eCos
ea
r
In Solar System
= r = a(1-e) minimum distance, perihelion
- = 1800 r = a(1+e) maximum distance, aphelion
Kepler-1
Kepler-2 rvrvSinvrh
The Orbit-2
Th O bit 3
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59
The Orbit-3
2
22
21 0
Eh
m
Eccentricity
(a)
(b)
(c)
(d)
m1 m1
m1m1
m2
m2 m2
m2
E=Kinetic Energy+Potential Energy
E = 0 , then e = 1 trajectory is parabolic
E < 0 , then e < 1 trajectory is ellips
E > 0 , then e > 1 trajectory ishiperbolic
2
2mEr
2
2
221
m
Ehe
Circle orbit
2
2
mE
a
Elliptic Orbit
2
2
mE
a
Hyperbolic Orbit
1 2( )G m m 2 1 21 1
2 ( )2
V G m mr a
Orbital characteristics of the planets
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Orbital characteristics of the planets
No Planet a[AU] P[y] e[.] P2/a3 Psin [d]
1 Mercury 0.387 0.241 0.206 1.002 115.9
2 Venus 0.723 0.615 0.007 1.001 583.95
3 Earth 1.000 1.000 0.017 1.000 -
4 Mars 1.524 1.881 0.093 1.000 780.012
5 Jupiter 5.203 11.86 0.048 0.999 393.85
6 Saturn 9.539 29.46 0.056 1.000 373.05
7 Uranus 19.19 84.07 0.046 1.000 369.65
8 Neptun
e
30.06 164.82 0.010 1.000 367.45
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Instability of Mercurys perihelion
I th U i f Ei t i
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In the Universe of Einstein Matter determines how space curves. Curved space determines how matter moves. Space & time cannot be separated: space-time Gravity is interaction between space-time and mass.
How to test Einstein?
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How to test Einstein?
Einsteins theory of gravity is called General relativity Gravity is weak! Compare to electrical force:
Need massive bodies!
Try astronomical bodies like planets & Sun!
Proton Electron
3910 1,000,000,000,000,000,000,000,000,000,000,000,000,000elc
grav
F
F
How to test Einstein?
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How to test Einstein?The first test: The precession of Mercurys orbit
General relativity theory can correctly predictprecession rate!
0.012 deg/century
One full rotation takes 3 million years!
P i d N t ti d t th
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Precession and Nutation: due to the
gravitational attractions of Sun and Moon
on the rotating,non-spherical Earth
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Sidereal Priode and Synodic Priode
Sidereal Priode : Time interval between
successive similar configurations of the object,
the Earth and the Star
Synodic Priode : Time interval betweensuccessive similar configurations of the object,
the Sun and the Earth. Example: opposition to
opposition, new moon to new moon
1 1 1
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Inferior Planet;
sin si
1 1 1
dP P P Superior Planet
Moonsin si
1 1 1
dP P P
Earths Psid = 365,25 days. Venus Psid= 224,7 days
Mars Psid =687 days. Moons Psid = 27,32 days
Venus Psin = 583,93 days
Moon Psin =29,53 days
Mars Psin=779,88 days= 780 days
sin si
1 1 1
dP P P
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sin si
1 1 1
dP P P
Moons Psin =29,53 days
Earths Psid = 365,25 days
Moons Psid = 27,32 days
Moons phase
1
12
q Cos
= phase angle= 180 q =0 new Moon
= 0 q = 1 Full Moon
= 90 q=0,5 Quarter moon
=0oMoons Phase
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O CBA
C
=180o
New Moon , q=0
SunFull Moon q=1
Moon
Earth
D
E
q = Ratio of brightness surface
OBCDE:ABCDE=AC':AB
1
12
q Cos
Moon s Phase
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Zodiac
Constellations for Southern Hemisphere
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Constellations for Southern Hemisphere
Summer Winter
Night and day
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Night and day
0Cost Tg Tg
t0half arc of day
-Suns declination
-observers latitude
Cases;
Observer at equator=00 t0= 900 arc
of day = 1800=12 jam
Sun at equator=00 t0= 900 arc of
day = 1800=12 jam
Observer at pole =900 and 00 t0 -
undefinition, arc day so no
Sunrise/Sunset
Planet and Satellite
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PlanetNamed by
the IAU
Provisionally
NamedTotal Moons
Mercury 0 0 0
Venus 0 0 0
Earth 1 0 1
Mars 2 0 2
Jupiter 38 25 63
Saturn 35 21 56
Uranus 27 0 27Neptune 9 4 13
Total Moons 112 50 162
Body TypeNamed by
the IAU
Provisionally
Named
Total objects
Known Dwarf Planets 2 1 3
Dwarf Planet Watch List 6 6 12
Grand Total 120 57 177
Data Mercur Venu Earth Mars Jupiter Saturn Uranu Neptun
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y s s e
r[au] 0,387 0,723 1 1,524 5,203 9,539 19,18 30,06
Po[d] 0,29 0,61 1 1,88 11,86 29,46 84,01 164,8
Pr[d] 59 243 1 1,03 0,41 0,44 0,68 0,83
V 1,61 1,17 1 0,81 0,44 0,32 0,23 0,18
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Earths magnetic field
mscf.nasa.gov
G h Eff t i V
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Greenhouse Effect in Venus
physics.uoregon.edu
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From Meteoroid To
Meteorite
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Story of Meteorite
Meteoroids
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Meteoroids
Scientists estimate that 1,000 tons to more than 10,000tons of meteoritic material falls on the Earth each day.
However, most of this material is very tiny - in the form of
micrometeoroids or dust-like grains a few micrometers in
size. (These particles are so tiny that the air resistance is
enough to slow them sufficiently that they do not burn up,
but rather fall gently to Earth.)
Where do they come from? They probably come from
within our own solar system, rather than interstellar
space. Their composition provides clues to their origins.
They may share a common origin with the asteroids.
Some meteoritic material is similar to the Earth and Moon
and some is quite different. Some evidence indicates an
origin from comets.
Solar WindFlows out from the corona
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Earths
magnetosphere
Continuously, in all directions Impacts Earths magnetic field
Image credit: K. Endo, Nikkei Science Inc.
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SEAMEO CENTRE FOR QITEP IN SCIENCE
The Heliosphere
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The Heliosphere
Beyond Our Solar System
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Beyond Our Solar SystemIn 1991, the nine worlds of our own solar system were the only known planets.
Astronomers did not believe that ourSun's environment was the only planet
producer in the universe. But they had no evidence of planets outside our solarsystem.
How quickly things change.
In 1991 radio astronomers detected the first extra solar planets orbiting a dying
pulsar star. Although the deadly radiation from the pulsar is not condusive to life,it was the first example of a star other than our Sun producing planets.
Since then more than 100 planets have been found orbiting other stars. Some of
them are orbiting extremely close to their parent star like the 51 Pegasi
planetary system, while others are found to be at distances comparable to
where Mars and Jupiterorbit in our solar system.Since then more than 100 planets have been found orbiting other stars. Some of
them are orbiting extremely close to their parent star like the 51 Pegasi
planetary system, while others are found to be at distances comparable to
where Mars and Jupiterorbit in our solar system.
83
http://solarsystem.nasa.gov/planets/profile.cfm?Object=Sunhttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Marshttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Jupiterhttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Marshttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Jupiterhttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Jupiterhttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Marshttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Jupiterhttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Marshttp://solarsystem.nasa.gov/planets/profile.cfm?Object=Sun -
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85 THANK YOUTSE-TSE
MERCY
DANKEGRACY
ARIGATO KOZAIMAS